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In the JCMT-Transient Survey Gregory J. Herczeg (ဂᵮྈ Shěn Léigē )

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In the JCMT-Transient Survey Gregory J. Herczeg (ဂᵮྈ Shěn Léigē ) Transients! in the JCMT-Transient Survey Gregory J. Herczeg (ဂᵮྈ Shěn Léigē ) Kavli Institute for Astronomy and Astrophysics, Peking University Transient Team Coordinators Others Gregory Herczeg (PI; PKU/China) Steve Mairs (Victoria), Hyunju Yoo (Chungnam), Doug Johnstone (co-PI; NRC/Canada) Kevin Lacaille (Dalhousie), Sung-ju Kang (KASI), Jeong-Eun Lee (KHU/Korea) Graham Bell (EAO), Sarah Graves (EAO), Yuri Aikawa (Tsukuba/Japan) Harriet Parsons (EAO), E’lisa Lee (EAO), Satoko Takahashi (NAOJ), Wen-Ping Chen Geoff Bower (ASIAA/Taiwan) (NCU) Miju Kang (KASI), James Lane Vivien Chen (NTU/Taiwan) (Victoria), Helen Kirk (NRC), Oscar Morata Jennifer Hatchell (Exeter/UK) (ASIAA), and many others (55 people total) Protostellar Evolution Cartoon from van Boekel 2005 Stars grow during protostellar phase Ltot=Lacc+Lphot Scattered by dust Cartoon from Isella 2006 Cartoon from Tobin+2012 Spectral Energy Distribution Measure Tbol (~peak of SED) and Lbol (luminosity) Enoch+2009 Luminosity Problem (Kenyon et al. 1990; Dunham et al. 2009) Evolutionary Class No disk Disk Class I Class 0 BolometricLuminosity Bolometric Temperature Episodic bursts of accretion (Kenyon et al. 1990; Dunham, Evans, et al. 2009) Steady accretion Episodic accretion Time dependence needed; episodic accretion is likely (but not only) solution (e.g., Offner & McKee; see review by Hartmann, Herczeg, & Calvet 2016). FUor and EXor outbursts (adapted from Kospal+2011) Decades-long FUor bursts: Gravitational instabilities in disk Months-long EXor bursts Magnetic instabilities in inner disk Accretion Variability: EX Lup 11 1893 14 1941 McLaughlin 1946 EX Lup: 1950-2008 2008 Outburst of EX Lup (Aspin+2010) • 5-magnitude brightness -7 – 2 x 10 Msol/yr – 100 times higher than quiescence • Lasted about half a year – Similar strength, duration as 1955 outburst Cartoon from Hartmann, Herczeg, & Calvet 2016, ARAA FUors: accretion rate is so large that magnetosphere gets crushed Causes of outbursts • Disk instabilities (universal) • Gravitational, magneto-rotational, thermal • Binarity (e.g. Bonnell & Bastien 1992, Reipurth 2000) • Magnetospheric instabilities (D’Angelo & Spruit 2010, Armitage 2016) • Tidal disruption of planets or alien weaponry (Herczeg+2016) Frequency: 1 of 104 stars from optical (Hillenbrand & Findeisen 2015) Models from Dunham & Vorobyov (2012) See also, e.g., Zhu+, Bae+, Stamatellos+, Vorobyov+, Machida+, others Protostars: bury accretion outburst in an envelope Era of Transient Surveys (ASAS-SN, PTF, Gaia, LSST) Accretion bursts in youngest stages of stellar growth: Not detectable in optical, near-IR surveys Episodic bursts of accretion (Kenyon et al. 1990; Dunham, Evans, et al. 2009) Steady accretion Episodic accretion Time dependence needed; episodic accretion is likely (but not only) solution (e.g., Offner & McKee; see review by Hartmann, Herczeg, & Calvet 2016). Evidence for episodic accretion ● Outbursts on more evolved protostars (FUors, EXors) ● Repeated jet shocks ● Chemical signatures of past epochs of high luminosity (e.g., Kim+2011; Jorgensen+2013) ● Models of disk instabilities Jet shocks of YSOs (Reipurth 1989; Hartigan+2011; Plunkett+2015) Evidence for episodic accretion: envelope chemistry+snow line Evidence for episodic accretion: envelope chemistry+snow line Jørgensen et al. 2015; see also, e.g., J.-E.Lee 2007 Envelope snow line and past variability Jørgensen et al. 2015 Evidence for episodic accretion ● Outbursts on more evolved protostars (FUors, EXors) ● Repeated jet shocks ● Chemical signatures of past epochs of high luminosity (e.g., Kim+2011; Jorgensen+2013) Models from Dunham & Vorobyov (2012) ● Models of disk See also, e.g., Zhu+, Bae+, Stamatellos+, Vorobyov+, instabilities Machida+, others How to detect protostellar variability? (adapted from Kospal+2011) Decades-long FUor bursts: Gravitational instabilities in disk Months-long EXor bursts Magnetic instabilities in inner disk Direct detection of protostellar variability? ASIAA Conference hosted by Sienny Shang in 2011 Radiative transfer: a burst through an envelope (Johnstone et al. 2013) Ltot=Lacc+Lphot Scattered by dust Luminosity burst heats the dust; flux increase at 850 microns caused by dust temperature Time delay: a few weeks (mostly light travel time) Light travel time smooths bursts ● Sub-mm continuum emission produced by dust ● Depends on dust Temp ● Luminosity burst heats up dust, increases sub-mm emission ● Timescale for energy to propagate through envelope: weeks Observed protostellar variability (Safron, Fischer, et al. 2015) Embedded source identified in mid-IR Spitzer; Strong sub-mm emission post-outburst Program description (Herczeg+subm; Mairs+accepted, Yoo+, Mairs+, Johnstone+ in prep) ● 150 total hours spread over 8 fields of 30 arcmin (1.6 sq deg) ● Perseus (2), Oph (1), Orion (3), Serpens (2) ● Roughly monthly monitoring ● Previous GBS epoch ● 105 bright clumps with ~200 protostars in fields Levels of accretion variability for MRI+GI instabilities (Bae+2014, green) and GI (Vorobyov & Basu 2010, red) ● 30’ Pong Data Calibration: spatial offsets (Mairs+accepted) Some points are 5” off; calibration reduces uncertainties to <1”. Measure offset of every observation, re-reduce to same pixel scale Flux calibration through differential photometry (Mairs+ 2017) Source 2/ 1 Observation Number Flux calibration with differential photometry (Mairs+2017) Default flux calibration uncertainty: 8% rms Relative flux (see also Dempsey+2013) uncertainty: ~2.5% A sub-mm Transient! Yoo, Lee, Mairs et al., in prep A sub-mm Transient! Behind the Sun the Behind Noise-dominated uncertainty Calibrators on bottom: ~2-3% accuracy The First JCMT Protostellar Variable Hodapp+1999, 2012: periodic near-IR variability with 543 d period Possible explanation: 1.5 yr eccentric binary Comparison to Gould Belt Survey: ~3-yr baselines (Mairs+ in prep; Johnstone+ in prep) GBS Data Transient Data Average GBS Point Average Transient Point ~few years Observation Number A 2nd JCMT Transient? *** PRELIMINARY *** Mairs+ in prep Transient Data GBS Data Average GBS Point Average Transient Point ~few years Observation Number Future of JCMT Transient Survey 3 Years, Began: 12/2015 250 Protostars,Deepest 1400 submillimetre Disk Sources maps of these regions by a factor of 2.5 Slide prepared by Mairs The Transient Future ● Survey continues through 2018B ● Identify more transients ● Also at 450 microns ● Follow up transients (already JCMT, SMA, ALMA proposals) ● Long-term variability? Noise-dominated uncertainty ● Full statistical analyses of fields ● Modelling effort ● Leverage depth for disk, filament, and VeLLO science.
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